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Table 3:

Parameters that have been used to obtain the best fit between the observed CMD and the BaSTI isochrones.
ID (m-M)0 $\it {E(B-V)}$ Z Age (Myr) $\Delta_{\rm {age}}$
ESO057-SC075 18.46 0.14 0.008 1400-1600 $200\pm50$
HODGE7 18.48 0.04 0.008 1400-1550 $150\pm50$
IC2146 18.50 0.07 0.008 1550 <50
NGC 1644 18.48 0.01 0.008 1550 <50
NGC 1652 18.48 0.06 0.008 1700 <50
NGC 1751 18.45 0.22 0.008 1300-1500 $200\pm50$
NGC 1783 18.46 0.06 0.008 1400-1600 $200\pm50$
NGC 1795 18.45 0.10 0.008 1300 <50
NGC 1806 18.44 0.09 0.008 1400-1600 $200\pm50$
NGC 1846 18.49 0.09 0.008 1350-1600 $250\pm50$
NGC 1852 18.50 0.08 0.008 1200-1450 $250\pm50$
NGC 1917 18.48 0.08 0.008 1200-1350 $150\pm50$
NGC 1978 18.49 0.09 0.008 2000 <100
NGC 1987 18.40 0.04 0.010 950-1200 $250\pm50$
NGC 2108 18.40 0.21 0.010 950-1100 $150\pm50$
NGC 2154 18.48 0.04 0.008 1350-1500 $150\pm50$

Source LaTeX | All tables | In the text

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